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The winds from HL Tau
Klaassen, P. D.; Mottram, J. C.; Maud, L. T.; Juhasz, A.
AA(UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK ), AB(Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands; Max-Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany), AC(Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands), AD(Institute of Astronomy, Madingley Road, Cambridge CB3 OHA, UK)
Monthly Notices of the Royal Astronomical Society, Volume 460, Issue 1, p.627-633 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
techniques: interferometric, stars: formation, stars: winds, outflows, ISM: jets and outflows, submillimetre: ISM
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


Outflowing motions, whether a wind launched from the disc, a jet launched from the protostar, or the entrained molecular outflow, appear to be a ubiquitous feature of star formation. These outwards motions have a number of root causes, and how they manifest is intricately linked to their environment as well as the process of star formation itself. Using the Atacama Large Millimeter/submillimeter Array (ALMA) Science Verification data of HL Tau, we investigate the high-velocity molecular gas being removed from the system as a result of the star formation process. We aim to place these motions in context with the optically detected jet, and the disc. With these high-resolution (˜1 arcsec) ALMA observations of CO (J=1-0), we quantify the outwards motions of the molecular gas. We find evidence for a bipolar outwards flow, with an opening angle, as measured in the redshifted lobe, starting off at 90°, and narrowing to 60° further from the disc, likely because of magnetic collimation. Its outwards velocity, corrected for inclination angle is of the order of 2.4 km s-1.
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